General properties of the DGS dwarf subsample.
|Galaxy||Coordinates||Dist.||Optical size||Metallicity||M B||M H I||L TIR||L Hα||L FUV|
|Haro 11||00h36′52.5′′||–33°33′19′′||92||0.4′× 0.5′||8.20(a)||–20.6||0.5(b)||185||92||22|
|(11 kpc × 13 kpc)|
|Mrk 1089||05h01′37.8′′||–04°15′28′′||57||0.6′× 0.2′||8.10||–20.5||24||34.3||23||–|
|(10 kpc × 3 kpc)|
|Mrk 930||23h31′58.3′′||+28°56′50′′||78||0.4′× 0.4′||8.03||–19.5||3.0||18.8||23||–|
|(9 kpc × 9 kpc)|
|NGC 4861||12h59′02.3′′||+34°51′34′′||7.5||4.0′× 1.5′||7.89||–16.8||0.48||0.323||0.04||0.46|
|(9 kpc × 3 kpc)|
|NGC 625||01h35′04.6′′||–41°26′10′′||3.9||5.8′× 1.9′||8.22||–16.2||0.13||0.280||0.18||0.11|
|(7 kpc × 2 kpc)|
|UM 311||01h15′34.0′′||–00°51′32′′||24||0.1′× 0.1′||8.38||–19.2||3.0||5.18||0.48||–|
|(0.7 kpc × 0.7 kpc)|
Notes. Coordinates and optical sizes are taken from the NASA/IPAC Extragalactic Database. The size of UM 311 is that of the individual H ii galaxy, but the complex that we consider is larger (~3′ × 2′). Distances, metallicities, MB, and H i masses are from (Madden et al. 2013, see references therein). For Mrk 930, MB is from Markarian et al. (1989). Luminosities and masses are scaled to the quoted distances. LTIR is the total infrared (TIR) luminosity measured by integrating SEDs from 8 to 1000μm, from Rémy-Ruyer et al. (in prep.).
For Haro 11, we keep the metallicity used in Cormier et al. (2012).
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